The galactic abundance gradients traced by B-type stars

Details The galactic abundance gradients traced by B-type stars The galactic abundance gradients traced by B-type stars

Sep 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...289..740k&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 289, no. 3, p. 740-748

Astronomy and Astrophysics

Astrophysics

67

Abundance, B Stars, Galactic Evolution, H Ii Regions, Main Sequence Stars, Milky Way Galaxy, Open Clusters, Stellar Spectra, Balmer Series, Local Thermodynamic Equilibrium, Metallicity, Spectrum Analysis, Stellar Spectrophotometry

Scientific paper

We obtained high S/N, high resolution spectra of 16 B-type main sequence stars in young open clusters and in H II regions with galactocentric distances between 7 and 16 kpc. Chemical abundances for this sample were derived using line-blanketed Local Thermodynamic Equilibrium (LTE) model atmospheres and line formation in LTE. Our analyses together with published data from similar analyses of B-type stars result in flat gradients or even no gradients at all for oxygen and nitrogen in the outer part of the galactic disk. It is conjectured that the larger metallicity gradients cited for H II regions are essentially due to a steepening within the inner 6 kpc towards the galactic center.

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